2018MNRAS.477.4915O

We present the first results of applying Gaussian Mixture Models in the stellar kinematic space of normalized angular momentum and binding energy on NIHAO high-resolution galaxies to separate the stars into multiple components. We exemplify this method, using a simulated Milky Way analogue, whose stellar component hosts thin and thick discs, classical and pseudo bulges, and a stellar halo. The properties of these stellar structures are in good agreement with observational expectations in terms of sizes, shapes, and rotational support. Interestingly, the two kinematic discs show surface mass density profiles more centrally concentrated than exponentials, while the bulges and the stellar halo are purely exponential. We trace back in time the Lagrangian mass of each component separately to study their formation history. Between z ∼ 3 and the end of halo virialization, z ∼ 1.3, all components lose a fraction of their angular momentum. The classical bulge loses the most (∼95per cent) and the thin disc the least (∼60per cent). Both bulges formed their stars in situ at high redshift, while the thin disc formed ∼98per centin situ, but with a constant SFR ∼ 1.5 M_☉ yr^–1 over the last ∼11 Gyr. Accreted stars (6per cent of total stellar mass) are mainly incorporated to the thick disc or the stellar halo, which formed ex situ 8per cent and 45per cent of their respective masses. Our analysis pipeline is freely available at https://github.com/aobr/gsf.